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Early neutron star evolution in high-mass X-ray binaries

Early neutron star evolution in high-mass X-ray binaries
Early neutron star evolution in high-mass X-ray binaries
The application of standard accretion theory to observations of X-ray binaries provides valuable insights into neutron star properties, such as their spin period and magnetic field. However, most studies concentrate on relatively old systems, where the neutron star is in its late propeller, accretor, or nearly spin equilibrium phase. Here we use an analytic model from standard accretion theory to illustrate the evolution of high-mass X-ray binaries early in their life. We show that a young neutron star is unlikely to be an accretor because of the long duration of ejector and propeller phases. We apply the model to the recently discovered ~4000 yr old high-mass X-ray binary XMMU J051342.6-672412 and find that the system's neutron star, with a tentative spin period of 4.4 s, cannot be in the accretor phase and has a magnetic field B > (a few)x10^13 G, which is comparable to the magnetic field of many older high-mass X-ray binaries and is much higher than the spin equilibrium inferred value of (a few)x10^11 G. The observed X-ray luminosity could be the result of thermal emission from a young cooling magnetic neutron star or a small amount of accretion that can occur in the propeller phase.
Accretion, Accretion discs, Pulsars: general, Stars: magnetic field, Stars: neutron, X-rays: binaries, X-rays: individual: XMMU J051342.6−672412
0035-8711
44-49
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Wijngaarden, M.J.P.
e6064827-8f6f-4fc4-b24d-140d11939237
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Tauris, Thomas M.
b88be86f-f82e-4b4b-a710-bd71a86f13ef
Haberl, F.
e279c877-e917-4a24-bcc9-cf7de12b33fb
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Wijngaarden, M.J.P.
e6064827-8f6f-4fc4-b24d-140d11939237
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Tauris, Thomas M.
b88be86f-f82e-4b4b-a710-bd71a86f13ef
Haberl, F.
e279c877-e917-4a24-bcc9-cf7de12b33fb

Ho, Wynn C.G., Wijngaarden, M.J.P., Andersson, Nils, Tauris, Thomas M. and Haberl, F. (2020) Early neutron star evolution in high-mass X-ray binaries. Monthly Notices of the Royal Astronomical Society, 494 (1), 44-49. (doi:10.1093/mnras/staa675).

Record type: Article

Abstract

The application of standard accretion theory to observations of X-ray binaries provides valuable insights into neutron star properties, such as their spin period and magnetic field. However, most studies concentrate on relatively old systems, where the neutron star is in its late propeller, accretor, or nearly spin equilibrium phase. Here we use an analytic model from standard accretion theory to illustrate the evolution of high-mass X-ray binaries early in their life. We show that a young neutron star is unlikely to be an accretor because of the long duration of ejector and propeller phases. We apply the model to the recently discovered ~4000 yr old high-mass X-ray binary XMMU J051342.6-672412 and find that the system's neutron star, with a tentative spin period of 4.4 s, cannot be in the accretor phase and has a magnetic field B > (a few)x10^13 G, which is comparable to the magnetic field of many older high-mass X-ray binaries and is much higher than the spin equilibrium inferred value of (a few)x10^11 G. The observed X-ray luminosity could be the result of thermal emission from a young cooling magnetic neutron star or a small amount of accretion that can occur in the propeller phase.

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2003.06436 - Accepted Manuscript
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Accepted/In Press date: 5 March 2020
e-pub ahead of print date: 13 March 2020
Published date: 30 March 2020
Additional Information: This article has been accepted for publication in Monthly Notices of Royal Astronomical Society ©: 2020 [The Authors] Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Keywords: Accretion, Accretion discs, Pulsars: general, Stars: magnetic field, Stars: neutron, X-rays: binaries, X-rays: individual: XMMU J051342.6−672412

Identifiers

Local EPrints ID: 438938
URI: http://eprints.soton.ac.uk/id/eprint/438938
ISSN: 0035-8711
PURE UUID: 6cfc6c49-3119-4835-ae7d-85d7c860ca2e
ORCID for Wynn C.G. Ho: ORCID iD orcid.org/0000-0002-6089-6836
ORCID for Nils Andersson: ORCID iD orcid.org/0000-0001-8550-3843

Catalogue record

Date deposited: 27 Mar 2020 17:30
Last modified: 26 Nov 2021 02:54

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Contributors

Author: Wynn C.G. Ho ORCID iD
Author: Nils Andersson ORCID iD
Author: Thomas M. Tauris
Author: F. Haberl

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